This concept of such a hot Jupiter around an M dwarf in a synchronized rotation is unique. Many studies addressing the correlation between the orbital period (\(P_\textnormal {orb}\) ) and the stellar rotation period (\(P_\textnormal {rot}\) ) have thus far been focused on more solar-like transiting host stars rather than M dwarfs, using Kepler data [1]}.
Findings from [2]} and [3]} suggest a clear absence of close-in planets (\(P_\textnormal {orb} \lesssim \)  2–3 days) around rapidly rotating stars (\(P_\textnormal {rot} \lesssim \)  5–10 days), where planets with shorter periods were nearly synchronous (\(P_\textnormal {orb} \sim P_\textnormal {rot}\) ).
[4]} proposed that the cause was orbital decay of close-in planets by their host stars. Besides, with regards to M dwarfs, [5]} showed that typical stellar rotation periods would often match the periods of planets in their habitable zone.
Regardless, there is a dearth of close-in massive planets around M dwarfs where only a handful of such are known, such as NGST-1 b [6]} or TOI-519 b [7]}. This is not a result of observational bias as these types of planets would be simple to detect through transits and precise RVs.
AD Leo was even used as a test case to check the effects of XUV irradiation on planet atmospheres [8]}, considering that the ionsphere can play an influential role in regulating the stability of upper atmospheres on giant planets.
Therefore, understanding the case of AD Leo could aid in finding the key methods for other potential planet detections that suffer from ambiguities due to 1:1 spin-orbit resonances.
